Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988esasp.281b.235j&link_type=abstract
In ESA, Proceedings of the Celebratory Symposium on a Decade of UV Astronomy with the IUE Satellite, Volume 2 p 235-237 (SEE N89
Astronomy and Astrophysics
Astronomy
7
Interstellar Extinction, Iue, Spaceborne Astronomy, Ultraviolet Astronomy, Ultraviolet Spectra, White Dwarf Stars, Absorption Spectra, Gas Ionization, Interstellar Gas, Line Spectra, Parameter Identification, Photoionization, Stellar Spectra
Scientific paper
A method of detecting and determining parameters for narrow absorption lines in IUE high-resolution spectra of hot white dwarfs was developed. It provides a statistical estimate of the variance of the parameters measured. The statistical accuracy of narrow line measurements with IUE spectra is discussed. The method was employed to determine the column densities of low-ionization species (including N I, Si II, and C II) in the line of sight to seven hot white dwarfs. High-ionization species (N V, Si IV, and C IV) are detected towards four of the stars. The temperature of the low-ionization gas towards 4 of the stars is constrained to be less than 50,000 K. The temperature of the high-ionization gas to two of the stars is constrained to be under 100,000 K, which is well below the equilibrium ionization temperature of a collisionally ionized gas. This suggests that this gas is either in a photoionized region (most likely near the star) or is produced in the photosphere of the star.
Basri Gibor
Bowyer Stuart
Jelinsky Patrick
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